The presence of type–C QPO and the broad-band spectral fitting at both epochs (E1 & E2) confirms that the power-law component dominates over the disk contribution, hence confirming the intermediate state of GRS 1716–249. Here, the soft photons from the accretion disk are Comptonized to higher energies via a hot corona of thermal electrons through the inverse Compton effect [1]}, [2]}. The two epochs have shown significant spectral changes leading to a successive softening of the source as inferred from the broad-band spectrum at E1 and E2. The broad Fe-K\(\alpha \)  line at 6.4 keV is an indication of a spinning black hole [3]}. The observed iron line is extended from nearly 6 to 8 keV along with a dip around 11 keV. This shows that both wings of the Fe-K\(\alpha \)  line are stretched. It is believed that the broadening of the red wing might be due to Doppler and General Relativity (GR) effects, while the blue wing is elongated because of scattering of the photons within the hot inner flow [4]}, [5]}, [6]}.
